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<H3><A NAME="SECTION00842200000000000000">
ANALYSE/ROMAFOT</A>
</H3>
<TT>ANALYSE/ROMAFOT</TT>
<FONT SIZE="-1"><TT>frame [cat_tab] [int_tab] [sigma,sat]</TT></FONT>
<P>
To examine the catalogue table created by the command <TT>FIND/ROMAFOT</TT>
one should use the command ``M'' followed by the sequential position of
the object. The commands ``W'', ``U'', ``6'', ``X'' and ``Y'' will set the
display.
<P>
A subframe with the selected star at the center is presented to the
user. This subframe can be reduced (or enlarged) by the command
``R'' followed by the decrement (or increment) in x and y: delta_x,
delta_y, respectively.
<P>
The command ``S'', followed by the shift in x and y coordinate
provokes the displacement of the window. ``R'' and ``S'' are useful
to include or exclude stars in the subframe.
<P>
A ``bar'' allows the display of the current status of the window.
<P>
The intensity profiles are displayed with a scale which saturates at
an intensity of
<!-- MATH: $I \simeq 950$ -->
<IMG
WIDTH="34" HEIGHT="20" ALIGN="BOTTOM" BORDER="0"
SRC="img213.gif"
ALT="$I \simeq 950$">.
This can be changed with the command
``B'' followed by a factor for the intensities, typically 0.1 or
smaller.
<P>
In crowded fields the maps, isophotal contours and intensity profiles
are not enough to visualize the situation. In this case the commands
``K'' and ``L'' may help. With ``K'' one gets the pixel coordinates
(both absolute in the frame and relative in the window) and the pixel
intensity at the cursor position. The command ``L'' gives the height
(above the background) at the vertical cursor position.
<P>
If the window has been properly set, shaped and understood,
the user is expected to position the cursor where he thinks a star
exists and give the command ``I''. This command passes the trial
position of the star and its height and will be repeated
for all the stars in the window. The maximum number of objects
allowed is 36, but the user is discouraged from approaching this
limit for many reasons. The most simple one is that 36 stars (i.e.
<!-- MATH: $36\times 3$ -->
<IMG
WIDTH="20" HEIGHT="39" ALIGN="MIDDLE" BORDER="0"
SRC="img214.gif"
ALT="$36\times 3$">
parameters) which are fitted separately in 36 subframes
with <I>N</I> pixels each require
<!-- MATH: $36 \times 3 \times N = 108 N$ -->
<IMG
WIDTH="149" HEIGHT="39" ALIGN="MIDDLE" BORDER="0"
SRC="img215.gif"
ALT="$36 \times 3 \times N = 108 N$">
calculations at each iteration: the same fit all together requires
<!-- MATH: $36 \times 3 \times 36 \times N = 3888 N$ -->
<IMG
WIDTH="208" HEIGHT="41" ALIGN="MIDDLE" BORDER="0"
SRC="img216.gif"
ALT="$36 \times 3 \times 36 \times N = 3888 N$">
calculations.
<P>
The command ``J'' works like ``I'' with the difference that the
user is expected to provide the trial value for the height: this
can be useful in case of difficult convergence when e.g. several
local minima exist in the parameter space.
<P>
If some unwanted feature is present in the window (cosmic rays,
scratches, tails of other stars and so on) ``E'' is most useful.
This command provokes a hole in the window whose radius will be
given by the operator. The hole is centered at the cursor position
and the pixels included within its area will be ignored in the
subsequent calculations as far as this window is concerned.
There is no effective limit to the number of holes <IMG
WIDTH="23" HEIGHT="42" ALIGN="MIDDLE" BORDER="0"
SRC="img217.gif"
ALT="$(\leq 50)$">.
For this reason, it is not practical to have hole positions
reported on the screen (in fact, they could fill the whole screen).
Therefore by default the holes will not be listed. To change that
use the command ``-'' which enables the report hole positions
and sizes. This command executes the inverse operation, as well.
<P>
During the examination of the objects passed by <TT>FIND/ROMAFOT</TT>
it often happens that several stars are asked to fit together in
the same window and some of these are in the catalogue table. In
order not to repeat photometry of the same objects,
<TT>ANALYSE/ROMAFOT</TT> flags in the catalogue table all the objects
already considered and the user is supplied with the message
``object already considered''. It is possible to disable this feature
with the key ``Z''.
<P>
The user may realize that the windows presented are too wide
(or too narrow) depending on the telescope scale, seeing, crowding
and so forth. In this case the command ``/'' can be used to change
the default window size.
<P>
A minor feature is the key ``A''. This allows the default display
of level contours (instead of colour maps) without using command
``X'' or ``Y''.
<P>
Finally, the command ``5'' selects the mode to examine the catalogue
table, either to give the record (manual mode
<!-- MATH: $\rightarrow$ -->
<IMG
WIDTH="52" HEIGHT="54" ALIGN="BOTTOM" BORDER="0"
SRC="img218.gif"
ALT="$\rightarrow$">
``M'')
or running through the table (automatic mode
<!-- MATH: $\rightarrow$ -->
<IMG
WIDTH="52" HEIGHT="54" ALIGN="BOTTOM" BORDER="0"
SRC="img219.gif"
ALT="$\rightarrow$">
``A'').
It is possible also to examine the list selectively (
<!-- MATH: $\rightarrow$ -->
<IMG
WIDTH="52" HEIGHT="54" ALIGN="BOTTOM" BORDER="0"
SRC="img220.gif"
ALT="$\rightarrow$">
``S''). For instance all the objects above a given height threshold
are disregarded by the command <TT>GROUP/ROMAFOT</TT>.
<P>
After execution of <TT>ANALYSE/ROMAFOT</TT> all the program stars
are arranged with their trial values in (normally multiple) windows
with selected dimensions and shapes: these data are stored in the
intermediate table. To continue the user should now run the command
<TT>FIT/ROMAFOT</TT>.
<P>
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<ADDRESS>
<I>Petra Nass</I>
<BR><I>1999-06-15</I>
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